TY - JOUR
T1 - Reversal or no reversal
T2 - The evolution of the star formation rate-density relation up to z ~ 1.6
AU - Ziparo, F.
AU - Popesso, P.
AU - Finoguenov, A.
AU - Biviano, A.
AU - Wuyts, S.
AU - Wilman, D.
AU - Salvato, M.
AU - Tanaka, M.
AU - Nandra, K.
AU - Lutz, D.
AU - Elbaz, D.
AU - Dickinson, M.
AU - Altieri, B.
AU - Aussel, H.
AU - Berta, S.
AU - Cimatti, A.
AU - Fadda, D.
AU - Genzel, R.
AU - Le Floc'h, E.
AU - Magnelli, B.
AU - Nordon, R.
AU - Poglitsch, A.
AU - Pozzi, F.
AU - Sanchez Portal, M.
AU - Tacconi, L.
AU - Bauer, F. E.
AU - Brandt, W. N.
AU - Cappelluti, N.
AU - Cooper, M. C.
AU - Mulchaey, J. S.
PY - 2014/1/1
Y1 - 2014/1/1
N2 - We investigate the evolution of the star formation rate (SFR)-density relation in the Extended Chandra Deep Field South and the Great Observatories Origin Deep Survey fields up to z ~ 1.6. In addition to the 'traditional method', in which the environment is defined according to a statistical measurement of the local galaxy density, we use a 'dynamical' approach, where galaxies are classified according to three different environment regimes: group, 'filamentlike' and field. Both methods show no evidence of an SFR-density reversal. Moreover, group galaxies show a mean SFR lower than other environments up to z ~ 1, while at earlier epochs group and field galaxies exhibit consistent levels of star formation (SF) activity. We find that processes related to a massive dark matter halo must be dominant in the suppression of the SF below z ~ 1, with respect to purely density-related processes. We confirm this finding by studying the distribution of galaxies in different environments with respect to the so-called main sequence (MS) of star-forming galaxies. Galaxies in both group and 'filament-like' environments preferentially lie below the MS up to z ~ 1, with group galaxies exhibiting lower levels of star-forming activity at a given mass. At z > 1, the star-forming galaxies in groups reside on the MS. Groups exhibit the highest fraction of quiescent galaxies up to z ~ 1, after which group, 'filament-like' and field environments have a similar mix of galaxy types. We conclude that groups are the most efficient locus for SF quenching. Thus, a fundamental difference exists between bound and unbound objects, or between dark matter haloes of different masses.
AB - We investigate the evolution of the star formation rate (SFR)-density relation in the Extended Chandra Deep Field South and the Great Observatories Origin Deep Survey fields up to z ~ 1.6. In addition to the 'traditional method', in which the environment is defined according to a statistical measurement of the local galaxy density, we use a 'dynamical' approach, where galaxies are classified according to three different environment regimes: group, 'filamentlike' and field. Both methods show no evidence of an SFR-density reversal. Moreover, group galaxies show a mean SFR lower than other environments up to z ~ 1, while at earlier epochs group and field galaxies exhibit consistent levels of star formation (SF) activity. We find that processes related to a massive dark matter halo must be dominant in the suppression of the SF below z ~ 1, with respect to purely density-related processes. We confirm this finding by studying the distribution of galaxies in different environments with respect to the so-called main sequence (MS) of star-forming galaxies. Galaxies in both group and 'filament-like' environments preferentially lie below the MS up to z ~ 1, with group galaxies exhibiting lower levels of star-forming activity at a given mass. At z > 1, the star-forming galaxies in groups reside on the MS. Groups exhibit the highest fraction of quiescent galaxies up to z ~ 1, after which group, 'filament-like' and field environments have a similar mix of galaxy types. We conclude that groups are the most efficient locus for SF quenching. Thus, a fundamental difference exists between bound and unbound objects, or between dark matter haloes of different masses.
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U2 - 10.1093/mnras/stt1901
DO - 10.1093/mnras/stt1901
M3 - Article
AN - SCOPUS:84890096099
SN - 0035-8711
VL - 437
SP - 458
EP - 474
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 1
ER -